In order to describe the structure of a static, non-rotating compact star, we
use the Tolman-Oppenheimer-Volkoff (TOV) equation for the pressure
\(p(r)\)  [1]}:
\(\frac{dp}{dr}=-\frac{\epsilon (r) M (r)}{r^2} \left[ 1 +\frac{p(r)}{\epsilon (r)} \right] \left[ 1 + \frac{4\pi r^3 p(r)}{M(r)}\right] \times \left[ 1 - \frac{2M(r)}{r} \right]^{-1}.\) 
